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opencc-by-4.0May 2020View details →

MVs and FVs for Planck 2015 and 2018 temperature maps obtained by polyMV

The files located in data_mvs.zip are the tables of Multipole Vectors (MVs) for Planck 2015 and 2018 temperature maps (full sky and masked maps using the Common Temperature mask of PR3). The files located in data_fvs.zip are the tables of Fréchet vectors (FVs) for Planck 2015 and 2018 temperature maps. MVs and FVs were obtained using <a href="https://oliveirara.github.io/polyMV/">polyMV</a>. Any publications making use of this data should cite this paper: R. A. Oliveira, T. S. Pereira, and M. Quartin, CMB statistical isotropy confirmation at all scales using multipole vectors, <a href="https://doi.org/10.1016/j.dark.2020.100608">Phys. Dark Univ. 30 (2020) 100608</a> (<a href="https://arxiv.org/abs/1812.02654">arXiv:1812.02654 [astro-ph.CO]</a>). Please refer to the above paper for further details.

opencc-by-4.0Sep 2020View details →

Sunyaev-Zeldovich Effect Tomography: Processed Planck Maps and Masks

This package contains two sets of products constructed and used in the Sunyaev-Zeldovich Effect Tomography project by Yi-Kuan Chiang, Ryu Makiya, Brice Ménard, and Eiichiro Komatsu. The first directory is a set of full-sky Planck HFI channel intensity maps from 100 to 353 GHz (Planck Collaboration 2016). We post-processed the maps to remove CMB fluctuations using that constructed in Bobin et al. (2016). The maps are stored using the HEALPix (Górski et al. 2005) scheme with the ring ordering of N_side = 2048. The map unit is MJy/sr. The second directory is a set of masks, including a 60% Galactic mask, a joint Planck point source mask, and a joint SDSS footprint and veto mask. The masks are in ring ordered HEALPix format of N_side = 2048. If you make use of these products, please cite the following papers: Chiang, Makiya, Ménard, & Komatsu, 2020, arXiv:2006.14650 Chiang, Makiya, Komatsu, & Ménard, 2020, arXiv:2007.01679

opencc-by-4.0Jan 2022View details →

Cosmological constraints from the tomographic cross-correlation of DESI Luminous Red Galaxies and Planck CMB lensing

Input maps and derived data for the DESI LRG samples, cross-correlated with the Planck CMB lensing maps, from Cosmological constraints from the tomographic cross-correlation of DESI Luminous Red Galaxies and Planck CMB lensing Martin White, et al. https://arxiv.org/abs/2111.09898

opencc-by-4.0Nov 2022View details →

Data supplement for: Validating the Nernst--Planck transport model under reaction-driven flow conditions using RetroPy v1.0

This is the repository for the publication's supplementary data and plotting scripts: Validating the Nernst–Planck transport model under reaction-driven flow conditions using RetroPy v1.0. The dependency of the scripts can be installed using conda and pip: <pre><code>conda create -n plot numpy matplotlib==3.6.1 h5py python=3.9 conda activate plot pip install palettable</code></pre> To reproduce the figures, execute the files using python: <pre><code>python figure03.py</code></pre>

opencc-by-4.0Jun 2023View details →

Figure scripts and output files from "How well do we understand the Planck feedback?"

Included is a readme file, MATLAB figure scripts, and the output files needed to make figures for Cronin & Dutta, 2023, JAMES.

zenodo24/100

Cross-Correlation of Planck CMB Lensing with DESI-Like LRGs: Derived Data Supplement

These are the derived data products from <a href="https://arxiv.org/abs/2010.04698">arXiv:2010.04698</a>. cluster_dndz gives the clustering-based galaxy redshift distribution, as described in Sec 3 and plotted in Fig 5. Cgg_Ckg_obs gives the binned power spectra (with magnification bias and noise terms already subtracted) and their errors, as described in Sec 4 and plotted in Figs 12 and 14.

opencc-by-4.0Oct 2020View details →

Planck Sunyaev-Zeldovich Cluster MMF1 List

The Planck Sunyaev-Zeldovich Cluster catalogs contain a list of galaxy clusters detected through the Sunyaev-Zel'dovich effect (SZ) and consist of candidate sources that were detected using multifrequency algorithms that use the distinct spectral signature of such clusters. This version of the SZ catalogs, a component of Planck Data Release 1, is derived from the data acquired by Planck between August 13 2009 and November 26 2010.Three pipelines are used to detect SZ clusters: two independent implementations of the Matched Multi-Filter (MMF1 and MMF3), and PowellSnakes (PwS). The main catalog is constructed as the union of the catalogs from the three detection methods. The individual catalogs are provided for the expert user in order to assess the consistency of the pipelines. The union catalogue contains the coordinates and the signal-to-noise ratio of the detections and a summary of the external validation information, including external identification of a cluster and its redshift if it is available.

Planck-ATCA Co-eval Observations (PACO) Project Bright Sample Catalog

The Planck Australia Telescope Compact Array (Planck-ATCA) Co-eval Observations (PACO) have provided flux density measurements of well-defined samples of Australia Telescope 20-GHz (AT20G) radio sources at frequencies below and overlapping with Planck frequency bands, almost simultaneously with Planck observations. The authors have observed with the ATCA a total of 482 sources in the frequency range between 4.5 and 40 GHz in the period between 2009 July and 2010 August. Several sources were observed more than once. In their paper, the authors present the aims of the project, the selection criteria, and the observation and data reduction procedures. They also discuss the data in total intensity for a complete sample of 189 sources with 20-GHz flux densities > 500 mJy, Galactic latitude |b| > 5 degrees and Declination < -30 degrees, and some statistical analysis of the spectral behavior and variability of this sample, referred to as the 'bright PACO sample'. Finally, the authors discuss how these data could be used to transfer absolute calibrations to ground-based telescopes using the cosmic microwave background dipole calibrated flux densities measured by the Planck satellite, and they provide some test fluxes on bright calibrators. This table contains the catalog of 1004 observations of 180 of the 189 sources that comprise the 'bright PACO sample'. Thus, each row in this table corresponds to a specific observation of a source, and there can be several rows for any source, corresponding to different observations. The ATCA observations were made in 6 2-GHz wide observing bands: 4732 - 6780 MHz, 8232 - 10280 MHz, 17232 - 19280 MHz, 23232 - 25280 MHz, 32232 - 34280 MHz and 38232 - 40280 MHz. In order to properly define the detailed source spectral behavior, the authors have split each 2-GHz band into 4 x 512 MHz sub-bands, and calibrated each sub-band independently. Thus, for each observation, the flux density at 24 frequencies is given. The frequency identifier in the flux density appears (at least to this HEASARC scientist) to be the lower frequency of the sub-band rather than its central frequency. In order to provide the easiest way to extrapolate the observed counts or model predictions from one frequency to another, the authors have modeled the observed source spectra. As their observations covered a wide frequency range from 4.5 to 40 GHz over which a single power law is not enough to describe the spectral behavior of the sources, they studied the spectra of the 174 point-like sources in this sample by fitting the observed data with a double power law of the form Snu = S0/[(nu/nu0)-a + (nu/nu0)-b], where nu is the frequency, Snu is the flux density in Jy, and S0, nu0, a and b are free parameters. The authors considered only those sources for which they had at least four data points for each of the 2 x 2 GHz bands considered. Full details of the fitting procedure are given in Section 3.1 of the reference paper. This table was created by the HEASARC in January 2014 based on the machine-readable version of Table S1 from the reference paper which was obtained from the CDS (their catalog J/MNRAS/415/1597 file table1.dat). This is a service provided by NASA HEASARC .

Planck Catalog of 30-GHz Compact Sources (PCCS) Release 2

Planck was a European Space Agency (ESA) mission, with significant contributions from the National Aeronautics and Space Agency (NASA). It was the third generation of space-based cosmic microwave background experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in orbit checkout, Planck initiated the First Light Survey on 12 August 2009. Planck then continuously measured the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 micron) with spatial resolutions ranging from about 33 to 5 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provided temperature and polarization information using radiometers which operated between 30 and 70 GHz. The High Frequency Instrument (HFI) used pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but did not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest Planck frequencies overlapped with WMAP, and the highest frequencies extended far into the submillimeter in order to improve separation between Galactic foregrounds and the cosmic microwave background (CMB). By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck provided an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Second Planck Catalogue of Compact Sources is a list of discrete objects detected in single-frequency maps from the full duration of the Planck mission and supersedes previous versions. It consists of compact sources, both Galactic and extragalactic, detected over the entire sky. Compact sources detected in the lower frequency channels are assigned to the PCCS2, while at higher frequencies they are assigned to one of two subcatalogs, the PCCS2 or PCCS2E, depending on their location on the sky. The first of these (PCCS2) covers most of the sky and allows the user to produce subsamples at higher reliabilities than the target 80% integral reliability of the catalog. The second (PCCS2E) contains sources detected in sky regions where the diffuse emission makes it difficult to quantify the reliability of the detections. Both the PCCS2 and PCCS2E include polarization measurements, in the form of polarized flux densities, or upper limits, and orientation angles for all seven polarization-sensitive Planck channels. The improved data-processing of the full-mission maps and their reduced noise levels allow the authors to increase the number of objects in the catalog, improving its completeness for the target 80% reliability as compared with the previous versions, the PCCS and the Early Release Compact Source Catalogue (ERCSC). The Low Frequency Instrument (LFI) Data Processing Center (DPC) produced the 30, 44, and 70 GHz maps after the completion of eight full surveys (spanning the period from 12 August 2009 to 3 August 2013). In addition, special LFI maps covering the period 1 April 2013 to 30 June 2013 were produced in order to compare the Planck flux-density scales with those of the Very Large Array and the Australia Telescope Compact Array, by performing simultaneous observations of a sample of sources over that period. The High Frequency Instrument (HFI) DPC produced the 100-, 143-, 217-, 353-, 545-, and 857-GHz maps after five full surveys (from 2009 August 12 to 2012 January 11). As in the PCCS, the PCCS2 provides four different measures of the flux density for each source. They are determined by the source detection algorithm (DETFLUX), aperture photometry (APERFLUX), point spread function fitting (PSFFLUX), and Gaussian fitting (GAUFLUX). Only the first is obtained from the filtered maps; the other measures are estimated from the full-sky maps at the positions of the sources. The source detection algorithm photometry, the aperture photometry, and the point spread function (PSF) fitting use the Planck band-average effective beams, calculated with FEBeCoP (Fast Effective Beam Convolution in Pixel space). Note that only the PSF fitting algorithm takes into account the variation of the PSF with position on the sky. The PCCS2 has been produced from the Planck full-mission maps (eight sky surveys in the LFI and five sky surveys in the HFI), and therefore supersedes the previous catalogs (for the PCCS only 1.5 surveys were analyzed). It also includes the latest calibration and beam information, and the authors have improved some of the algorithms used to measure the photometry of the sources. This table contains the PCCS Public Release 2 table of sources detected at 30 GHz. Where the HEASARC parameter names differ from those used in the original table, the original names are listed parenthetically in upper case at the end of the parameter description. This table w

Planck Catalog of Compact Sources 857GHz Catalog

The Planck Catalogue of Compact Sources (PCCS) is a sample of reliable sources, both Galactic and extragalactic, extracted directly from the Planck nominal maps. The first public version of the PCCS, a component of Planck Data Release 1, is derived from the data acquired by Planck between August 13 2009 and November 26 2010. The PCCS consists of nine lists of sources, extracted independently from each of Planck's nine frequency channels. The source lists contain 24 columns per source at the LFI and HFI bands. The 857 GHz source list has six additional columns which give the flux densities and flux density uncertainties at the three adjacent lower frequencies: 217, 353, and 545 GHz.

Planck Sunyaev-Zeldovich Cluster UNION List

Planck PR2 Sunyaev-Zeldovich Cluster MMF1 List

These catalogs contain a list of galaxy clusters detected through the Sunyaev-Zel'dovich effect (SZ) and consist of candidate sources that were detected using multifrequency algorithms that use the distinct spectral signature of such clusters. This version of the SZ catalogs is a component of Planck Data Release 2.Three pipelines are used to detect SZ clusters: two independent implementations of the Matched Multi-Filter (MMF1 and MMF3), and PowellSnakes (PwS). The main catalog is the union of the catalogs from the three detection methods. The individual catalogs are provided for the expert user in order to assess the consistency of the pipelines. The union catalogue contains the coordinates and the signal-to-noise ratio of the detections and a summary of the external validation information, including external identification of a cluster and its redshift if it is available.